Therefore, we replaced the nthComp model by the self-consistent, broadband reflection model relxilllpCp from the relxill [1]}, [2]} model family, to account for the relativistic reflection spectrum. Thus, our best fit model is TBabs\(\times \) (diskbb+relxilllpCp). The relxilllpCp model is based on a lamp-post geometry of the corona, which is believed to be the illuminating source. In the lamp-post geometry, the corona is treated as a point source positioned at a height h, on the black hole spin axis above the accretion disk. The relxilllpCp model uses the thermal Comptonization model nthComp as the input continuum. In the case of the relxilllpCp model, the value of the reflection fraction (Refl\(_{frac}\) ) can be self-consistently determined, depending on the values of the lamp-post height (h), the black hole spin parameter (a\(^{*}\) ) and the inner accretion disk radius (R\(_{in}\) ) through ray-tracing calculations. The evaluation of Refl\(_{frac}\)  by the model itself helps to reduce the parameter space and eventually constrains the geometry of the system [2]}.
